J/A+A/445/673 X-ray spectrum of SV Cam (Sanz-Forcada+, 2006)
A compact flare eclipsed in the corona of SV Camelopardalis.
Sanz-Forcada J., Favata F., Micela G.
<Astron. Astrophys. 445, 673 (2006)>
=2006A&A...445..673S 2006A&A...445..673S
ADC_Keywords: Stars, variable ; Spectroscopy ; X-ray sources
Keywords: stars: coronae - stars: abundances - stars: individual: SV Cam -
stars: late-type - X-rays: stars - binaries: eclipsing
Abstract:
The eclipsing active binary SV Cam (G0V/K6V, Porb=0.593071d)
was observed with XMM-Newton during two campaigns in 2001 and 2003.
Description:
This table includes the observed fluxes of the lines identified in the
X-ray spectrum (XMM/RGS) of SV Cam. The table list the observed fluxes
at Earth, and a comparison with the fluxes predicted for a given
thermal coronal structure (the Emission Measure Distribution, EMD),
the emissivities provided by the Astrophysical Plasma Emission Model
(APED), and column density of absorbing material in the interstellar
medium towards the star. A list of the most important (at least a 5%
of the flux predicted for the line) blends that have been considered
for each line is included.
Objects:
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RA (2000) DE Designation(s)
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06 41 19.07 +82 16 02 SV Cam = HD 44982
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 116 53 XMM/RGS line fluxes of SV Cam (October 2003)
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See also:
J/A+A/406/193 : SV Cam BVR light curves in Feb/2001-Mar/2002 (Zboril, 2003)
J/A+A/376/158 : SV Cam BVR light curves (Albayrak+, 2001)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Ion Ion
10- 16 F7.4 0.1nm lambda Wavelength of the line as identified
in the model
18- 20 F3.1 [K] logTmax ? Maximum temperature of formation of
the line (unweighted by the EMD)
22- 29 E8.3 mW/m2 Fobs Observed line flux measured in XMM/RGS
SV Cam spectra
31- 34 F4.1 --- S/N Signal-to-noise ratio
36- 40 F5.2 --- log(Fobs/Fpred) ?=- Observed to predicted flux ratio (1)
42-116 A75 --- Blends Blends to the main line amounting more
than a 5% of the total flux (2)
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Note (1): Predicted flux includes correction by interstellar medium absorption.
Note (2): For a line not identified in APED, a tentative identification
is suggested in this column based on Kelly (1987aisl.book.....K 1987aisl.book.....K,
1897, Atomic and ionic spectrum lines below 2000 Angstroms. Hydrogen
through Krypton, New York: American Institute of Physics (AIP),
American Chemical Society and the National Bureau of Standards).
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Acknowledgements: Jorge Sanz-Forcada, jsanz(at)rssd.esa.int
(End) Jorge Sanz-Forcada [RSSD, ESA], Patricia Vannier [CDS] 05-Nov-2005